Constraints on dark matter self-interaction from galactic core size

Ray, Tirtha Sankar; Sarkar, Sambo; Shaw, Abinash Kumar

doi:10.48550/arxiv.2202.12247

Cited by 4 publications

(3 citation statements)

References 61 publications

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“…These simulations are often computationally expensive as they need a high resolution in order to resolve the central halo, where the dark matter collision rate is the highest. In some cases, controlled high-resolution Nbody simulations can be used to study SIDM predictions, see, e.g., [39][40][41][42][43][44][45][46]. A conducting fluid model is also broadly used [6-8, 24, 47-50], as it can resolve the central region of a collapsed halo, but the model is based on an idealized setup.…”

Section: Introductionmentioning

confidence: 99%

A parametric model for self-interacting dark matter halos

Yang,

Nadler,

et al. 2024

J. Cosmol. Astropart. Phys.

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We propose a parametric model for studying self-interacting dark matter (SIDM) halos. The model uses an analytical density profile, calibrated using a controlled N-body SIDM simulation that covers the entire gravothermal evolution, including core-forming and -collapsing phases. By normalizing the calibrated density profile, we obtain a universal description for SIDM halos at any evolution phase. The model allows us to infer properties of SIDM halos based on their cold dark matter (CDM) counterparts. As a basic application, we only require two characteristic parameters of an isolated CDM halo at z = 0. We then extend the model to incorporate effects induced by halo mass changes, such as major mergers or tidal stripping, making it applicable to both isolated halos and subhalos. The parametric model is tested and validated using cosmological zoom-in SIDM simulations available in the literature.

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Section: Introductionmentioning

confidence: 99%

A parametric model for self-interacting dark matter halos

Yang,

Nadler,

et al. 2024

J. Cosmol. Astropart. Phys.

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“…SIDM particle candidates are readily predicted by 'hidden sector' particle physics models and can potentially resolve the ΛCDM small scale challenges [12][13][14][15][25][26][27][28][29][30][31]. Self-interactions transport heat from the hotter outer halo to the JCAP02(2023)040 inner cooler halo leading to the transformation of higher density cusps into lower density cores [32][33][34]. Furthermore, SIDM subhalos are less concentrated than their CDM counterparts and are therefore more prone to tidal disruption, leading to a reduced subhalo mass function [35,36].…”

Section: Introductionmentioning

confidence: 99%

The local dark matter distribution in self-interacting dark matter halos

Rahimi

Vienneau²,

Bozorgnia³

et al. 2023

J. Cosmol. Astropart. Phys.

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We study the effects of dark matter self-interactions on the local dark matter distribution in selected Milky Way-like galaxies in the EAGLE hydrodynamical simulations. The simulations were run with two different self-interacting dark matter models, a constant and velocity-dependent self-interaction cross-section. We find that the local dark matter velocity distribution of the Milky Way-like halos in the simulations with dark matter self-interactions and baryons are generally similar to those extracted from cold collisionless dark matter simulations with baryons. In both cases, the local dark matter speed distributions agree well with their best fit Maxwellian distributions. Including baryons in the simulations with or without dark matter self-interactions increases the local dark matter density and shifts the dark matter speed distributions to higher speeds. To study the implications for direct detection, we compute the dark matter halo integrals obtained directly from the simulations and compare them to those obtained from the best fit Maxwellian velocity distribution. We find that a Maxwellian distribution provides a good fit to the halo integrals of most halos, without any significant difference between the results of different dark matter self-interaction models.

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“…In particular, density cores have been studied in the literature and used to constrain self-interactions (e.g. Correa 2021;Sagunski et al 2021;Ray et al 2022). Recent strong lensing observations provide further evidence for DM cores in galaxy clusters(Limousin et al 2022).In cosmological simulations of rSIDM density and circular velocity profiles of haloes have been studied previously byRocha et al (2013);Robertson et al (2019);Banerjee et al (2020);Stafford et al (2020).…”

mentioning

confidence: 99%

Cosmological simulations with rare and frequent dark matter self-interactions

Fischer

Brüggen

Schmidt-Hoberg

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Dark matter (DM) with self-interactions is a promising solution for the small-scale problems of the standard cosmological model. Here we perform the first cosmological simulation of frequent DM self-interactions, corresponding to small-angle DM scatterings. The focus of our analysis lies in finding and understanding differences to the traditionally assumed rare DM (large-angle) self scatterings. For this purpose, we compute the distribution of DM densities, the matter power spectrum, the two-point correlation function and the halo and subhalo mass functions. Furthermore, we investigate the density profiles of the DM haloes and their shapes. We find that overall large-angle and small-angle scatterings behave fairly similarly with a few exceptions. In particular, the number of satellites is considerably suppressed for frequent compared to rare self-interactions with the same cross-section. Overall we observe that while differences between the two cases may be difficult to establish using a single measure, the degeneracy may be broken through a combination of multiple ones. For instance, the combination of satellite counts with halo density or shape profiles could allow discriminating between rare and frequent self-interactions. As a by-product of our analysis, we provide - for the first time - upper limits on the cross-section for frequent self-interactions.

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Constraints on dark matter self-interaction from galactic core size

Cited by 4 publications

References 61 publications

A parametric model for self-interacting dark matter halos

A parametric model for self-interacting dark matter halos

The local dark matter distribution in self-interacting dark matter halos

Cosmological simulations with rare and frequent dark matter self-interactions

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